Optimizing a Pulsar Timing Array

Details Optimizing a Pulsar Timing Array Optimizing a Pulsar Timing Array

Jan 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21713904s&link_type=abstract

American Astronomical Society, AAS Meeting #217, #139.04; Bulletin of the American Astronomical Society, Vol. 43, 2011

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Scientific paper

Nanohertz gravitational radiation can be detected through the long term analysis of pulse arrival times from a set of millisecond pulsars (a pulsar timing array). The sources of this emission include inspiraling massive black hole binaries and cosmic strings.
Here, we assess the sensitivity of pulsar timing arrays to gravitational waves in the presence of a diverse range of noise sources both intrinsic and extrinsic to the pulsar.
Noise sources intrinsic to the pulsar include terms associated with pulsar rotational irregularities (timing noise) and jitter of the radio emission region. Extrinsic noise includes terms associated with reflex motion of the pulsar about unmodeled circumpulsar asteroid belts and propagation of the pulsar radio emission through turbulent plasma in the interstellar medium. We describe the amenability of these noise sources to various mitigation techniques, such as observing with higher sensitivity telescopes and multi-frequency time of arrival fitting.
We find that observations of more pulsars, observed with higher throughput (longer integrations times or faster observing cadences) are required to make a significant detection of gravitational radiation at cosmological levels and perform subsequent characterization of gravitational wave emitting sources. From this we conclude that pulsar timing is optimally conducted by using telescopes with a range of collecting areas, which can be achieved through coordinated global efforts utilizing current telescopes or a large array-based telescope.

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